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Abstract The behaviour of cool stars is largely governed by molecular absorptions in their outer atmospheres. At the temperatures involved (1000 -- 4000 K), the of transitions involved can be vast. The underlying physics of the is outlined and the status attempts to address the demands of stellar discussed. Progress on calculations of line lists for stellar models UCL is described. Specific examples of involving water, HCN/HNC, C₃, ₃⁺ and HDO are given. Outstanding needs are summarised.
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Tennyson et al. (2007) studied this question.
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